Download Silicon isotopic abundance toward evolved stars and its application

Astronomy
&
Astrophysics
A&A 559, L8 (2013)
DOI: 10.1051/0004-6361/201322466
c ESO 2013
Letter to the Editor
Silicon isotopic abundance toward evolved stars
and its application for presolar grains,
T.-C. Peng1 , E. M. L. Humphreys1 , L. Testi1,2,3 , A. Baudry4,5 , M. Wittkowski1 , M. G. Rawlings6 ,
I. de Gregorio-Monsalvo1,8 , W. Vlemmings7 , L.-A. Nyman8 , M. D. Gray9 , and C. de Breuck1
1
2
3
4
5
6
7
8
9
ESO Garching, Karl-Schwarzschild Str. 2, 85748 Garching, Germany
e-mail: [email protected]
Excellence Cluster Universe, Boltzmannstr. 2, 85748 Garching, Germany
INAF – Osservatorio Astrofisico di Arcetri, Largo E. Fermi 5, 50125 Firenze, Italy
Univ. Bordeaux, LAB, UMR 5804, 33270 Floirac, France
CNRS, LAB, UMR 5804, 33270 Floirac, France
National Radio Astronomy Observatory, 520 Edgemont Road, Charlottesville, VA 22903, USA
Department of Earth and Space Sciences, Chalmers University of Technology, Onsala Space Observatory, 439 92 Onsala, Sweden
Joint ALMA Observatory (JAO) and European Southern Observatory, Alonso de Córdova 3107, Vitacura, Santiago, Chile
JBCA, Alan Turing Building, School of Physics and Astronomy, University of Manchester, Manchester M13 9PL, UK
Received 9 August 2013 / Accepted 18 October 2013
ABSTRACT
Aims. Galactic chemical evolution (GCE) is important for understanding the composition of the present-day interstellar medium
(ISM) and of our solar system. In this paper, we aim to track the GCE by using the 29 Si/30 Si ratios in evolved stars and tentatively
relate this to presolar grain composition.
Methods. We used the APEX telescope to detect thermal SiO isotopologue emission toward four oxygen-rich M-type stars. Together
with the data retrieved from the Herschel science archive and from the literature, we were able to obtain the 29 Si/30 Si ratios for a
total of 15 evolved stars inferred from their optically thin 29 SiO and 30 SiO emission. These stars cover a range of masses and ages,
and because they do not significantly alter 29 Si/30 Si during their lifetimes, they provide excellent probes of the ISM metallicity (or
29
Si/30 Si ratio) as a function of time.
Results. The 29 Si/30 Si ratios inferred from the thermal SiO emission tend to be lower toward low-mass oxygen-rich stars (e.g., down
to about unity for W Hya), and close to an interstellar or solar value of 1.5 for the higher-mass carbon star IRC+10216 and two
red supergiants. There is a tentative correlation between the 29 Si/30 Si ratios and the mass-loss rates of evolved stars, where we take
the mass-loss rate as a proxy for the initial stellar mass or current stellar age. This is consistent with the different abundance ratios
found in presolar grains. Before the formation of the Sun, the presolar grains indicate that the bulk of presolar grains already had
29
Si/30 Si ratios of about 1.5, which is also the ratio we found for the objects younger than the Sun, such as VY CMa and IRC+10216.
However, we found that older objects (up to possibly 10 Gyr old) in our sample trace a previous, lower 29 Si/30 Si value of about 1.
Material with this isotopic ratio is present in two subclasses of presolar grains, providing independent evidence of the lower ratio.
Therefore, the 29 Si/30 Si ratio derived from the SiO emission of evolved stars is a useful diagnostic tool for the study of the GCE and
presolar grains.
Key words. ISM: abundances – stars: late-type – submillimeter: ISM – ISM: molecules
1. Introduction
As the eighth most abundant element in the Universe, silicon
plays an important role in understanding nucleosynthesis and
Galactic chemical evolution (GCE). The main isotope 28 Si is
mainly produced by early-generation massive stars that become
Type II supernovae. The other two stable isotopes 29 Si and 30 Si
are mainly produced by O and Ne burning in massive stars or
by slow neutron capture (the s-process) and by explosive burning in the final stages of stellar evolution, that is, the asymptotic
This publication is based on data acquired with the Atacama
Pathfinder Experiment (APEX). APEX is a collaboration between
the Max-Planck-Institut für Radioastronomie, the European Southern
Observatory, and the Onsala Space Observatory. Herschel is an ESA
space observatory with science instruments provided by European-led
Principal Investigator consortia and with important participation from
NASA.
Tables 2, 3, and Fig. 4 are available in electronic form at
http://www.aanda.org
giant branch (AGB) phase for low- and intermediate-mass stars
and supernova explosions for high-mass stars (see, e.g., Woosley
& Weaver 1995; Timmes & Clayton 1996; Alexander & Nittler
1999).
In the thermally pulsing AGB (TP-AGB) phase, thermonuclear runaways are periodically caused by He burning in a
thin shell between the H-He discontinuity and the electrondegenerate C-O core. This energy goes directly into heating
the local area and raises the pressure, which initiates an expansion and a series of convective and mixing events (Herwig
2005; Iben & Renzini 1983). During the so-called third dredgeup, the products of He burning and the s-process elements are
brought to the surface, e.g., 12 C, which can lead to the formation of S- (C/O ≈ 1) or C-type (C/O > 1) stars. In conjunction with dredge-ups, the Si-bearing molecules (e.g., SiC and
SiO) formed in the stellar surface eventually condense onto dust
grains or actually form dust grains. The silicon isotopic ratios
will be preserved and go through the journey in the interstellar
medium (ISM) until they are used again to form stars.
Article published by EDP Sciences
L8, page 1 of 6
A&A 559, L8 (2013)
Table 1. Spectral parameters of the observed SiO isotopologue
transitions.
Line
SiO υ = 0, J
SiO υ = 0, J
30
SiO υ = 0, J
29
SiO υ = 0, J
30
SiO υ = 0, J
29
SiO υ = 0, J
30
SiO υ = 0, J
28
29
= 6–5
= 6–5
= 6–5
= 7–6
= 7–6
= 26–25
= 26–25
Frequency
(MHz)
Eup /k
(K)
θMB
( )
Instrument
260 518.02
257 255.22
254 216.66
300 120.48
296 575.74
1 112 832.94
1 099 711.49
43.8
43.3
42.7
57.7
57.0
721.6
713.1
24.0
24.3
24.5
20.8
21.1
19.8
19.6
APEX-1
APEX-1
APEX-1
APEX-2
APEX-2
HIFI
HIFI
Notes. θMB is the FWHM beam width at the observed frequencies.
The Kelvin-to-Jansky conversions are 39, 41, and 390 Jy K−1 for the
APEX-1, 2, and HIFI observations, respectively.
AGB stars can produce almost all grains of interstellar dusts,
and their dust production is one order of magnitude higher
than that of supernovae in the Milky Way (see, e.g., Dorschner
& Henning 1995; Gehrz 1989). It is generally believed that
oxygen-rich M-type stars produce mainly silicate grains and
carbon-rich stars mainly carbonaceous grains (Gilman 1969).
However, the actual situation may be more complicated and
grain composition may change during the AGB phase (Lebzelter
et al. 2006).
The measured 29 Si/30 Si ratios in the ISM are about 1.5 (Wolff
1980; Penzias 1981), very close to that of the solar system
(Anders & Grevesse 1989; Asplund et al. 2009). However, nearinfrared SiO observations of Tsuji et al. (1994) showed that some
evolved stars have 29 Si/30 Si ratios slightly below 1.5. Our new
observations of SiO isotopologues in the radio domain with the
APEX and Herschel telescopes confirm the low 29 Si/30 Si ratios
for oxygen-rich M-type stars.
2. Observations
Observations of the SiO isotopologue lines toward VY CMa,
o Ceti, W Hya, and R Leo were carried out with the 12-m APEX
telescope in 2011 September and 2012 December on Llano de
Chajnantor in Chile. The single-sideband heterodyne receivers
APEX-1 and APEX-2 (Vassilev et al. 2008; Risacher et al.
2006) were used during the observations. The focus and pointing of the antenna were checked on Jupiter and Mars. The pointing and tracking accuracy were about 2 and 1 , respectively.
The extended bandwidth Fast Fourier Transform Spectrometer
(XFFTS; Klein et al. 2012) backend was mounted and configured into a bandwidth of 2.5 GHz and ∼0.1 km s−1 resolution.
In addition, the Herschel/HIFI data of VY CMa, o Ceti, W Hya,
χ Cyg, R Cas, and R Dor were retrieved from the Herschel science archive.
All spectra were converted to the main beam brightness temperature unit, T MB = T A∗ /ηMB (ηMB = Beff /Feff ), using the forward efficiencies (Feff ) and the beam-coupling efficiencies (Beff )
from the APEX documentation1. The beam efficiencies of HIFI
were taken from the Herschel/HIFI documentation webpage. We
adopted ηMB of 0.75, 0.73, and 0.76 for the APEX-1, 2, and
HIFI data, respectively. All data were reduced and analyzed by
using the standard procedures in the GILDAS2 package. The
1
2
http://www.apex-telescope.org
http://www.iram.fr/IRAMFR/GILDAS/
L8, page 2 of 6
Fig. 1. Left: APEX ground-vibrational 28 SiO (black), 29 SiO (red), and
30
SiO (blue) J = 6−5 spectra toward VY CMa, o Ceti, and W Hya.
The intensities of the 29 SiO and 30 SiO lines were multiplied by two
for clarity. Right: Herschel/HIFI ground-vibrational 29 SiO (red) and
30
SiO (blue) J = 26−25 spectra at around 1.1 THz toward the same
sources. The 29 SiO emission of VY CMa is blended by the 13 CO J =
10−9 line from the other sideband. The dashed lines indicate the VLSR
of the sources.
SiO spectroscopic data were taken from the Cologne database
for molecular spectroscopy (CDMS3 ) and are listed in Table 1.
3. Results and discussion
The APEX and Herschel SiO isotopologue spectra of the selected evolved stars (with both APEX and Herschel detections)
are shown in Figs. 1 and 4, and the SiO intensity measurements
are summarized in Table 2. The 29 SiO and 30 SiO emission is expected to be optically thin because the abundance of the main
isotopologue 28 SiO is at least ten times larger than 29 SiO in
the ISM (Penzias 1981). Additionally, the solar and terrestrial
29
Si/30 Si ratios are close to 1.5 (de Bièvre et al. 1984; Anders &
Grevesse 1989). The 29 SiO/30 SiO J = 26−25 intensity ratios observed with the Herschel/HIFI instrument for o Ceti and W Hya
(Fig. 1) are consistent with the low-J results obtained with the
APEX telescope. Fitting two Gaussian profiles to the 29 SiO line
and the partially blended 13 CO J = 10−9 line in the HIFI
VY CMa spectra, we obtained a 29 SiO/30 SiO J = 26−25 intensity ratio of 1.4 ± 0.1, also consistent with the low-J APEX data.
Because the upper-state energies Eup /k of J = 26−25 lines
are about 700 K higher than those of J = 6−5, the constant
29
SiO/30 SiO intensity ratio of low- and high-J transitions indicates optically thin 29 SiO and 30 SiO emission with similar distributions and excitation conditions. In addition, we believe that
the 29 SiO and 30 SiO emission obtained for our sample stars is unlikely to be dominated by masing effects due to the lack of any
narrow spectral features. Therefore, the 29 SiO/30 SiO intensity ratio directly reflects the abundance ratio between 29 Si and 30 Si in
the circumstellar envelopes of these stars, assuming any differences in chemical fractionation or photodissociation are minor.
The derived 29 Si/30 Si ratios are listed in Table 3.
3
http://www.astro.uni-koeln.de/cdms/
T.-C. Peng et al.: Silicon isotopic abundance toward evolved stars
Fig. 2. Comparison of 29 Si/30 Si in evolved stars. The dashed line
indicates the terrestrial and solar 29 Si/30 Si abundance ratio of 1.51
(de Bièvre et al. 1984; Anders & Grevesse 1989; Asplund et al. 2009).
The red line is a linear fit to the 29 Si/30 Si– Ṁ relation.
evolved stars. We note that the stars in our sample only trace
the 29 Si/30 Si ratio of their natal clouds if they do not modify this
ratio via nucleosynthesis (see, e.g., Zinner et al. 2006).
The second possibility for different 29 Si/30 Si ratios is that
the stars in the AGB phase can significantly modify these ratios.
Some of the M-type stars will become C-type stars after several
dredge-up episodes with higher mass-loss rates toward the end
of the AGB phase (see, e.g., Herwig 2005). If the 29 Si/30 Si ratio can be modified by the s-process in the He-burning shell in
evolved stars, it must be done efficiently because the AGB time
scale is short (a few times 106 yr, see Marigo & Girardi 2007).
However, the modeling results of Zinner et al. (2006) show that
the 29 Si/30 Si ratios of low-mass stars do not significantly change
during the AGB phase (see also the discussion of Decin et al.
2010).
3.2.
3.1. Silicon isotope ratios
Since 28 Si is mainly produced via the α-process in massive
stars, the 28 Si in low-mass stars comes from their natal clouds.
Additionally, stable isotopes 29 Si and 30 Si can be formed via
slow neutron capture (the s-process) in both low- and high-mass
stars. It has been shown by Timmes & Clayton (1996) that 28 Si is
the primary isotope in the GCE with a roughly constant siliconto-iron ratio over time, independent of the initial metallicity. On
the other hand, neutron-rich isotopes 29 Si and 30 Si show strong
dependence on the composition and initial metallicity.
In Fig. 2, the 29 Si/30 Si ratios derived from the SiO integrated
intensities are plotted against the mass-loss rates for different
evolved stars, and they show a tendency to increase with increasing mass-loss rates. The two supergiants VY CMa and NML Cyg
and the carbon star IRC+10216 have 29 Si/30 Si ratios close to the
solar value of 1.5. The rest of the samples (see also Table 3) have
29
Si/30 Si ratios <1.5, for example, the 29 Si/30 Si ≈ 1 for W Hya.
There are two possibilities for the different 29 Si/30 Si ratios seen
in our sample. One is that the silicon isotope ratios merely reflect
the initial chemical composition of the environment where these
stars were born and the different ratios are the results of different ages, which mainly depend on their masses and metallicities.
The other possibility is that the stellar evolution can significantly
change the silicon isotope ratios.
The first possibility implies that the 29 Si/30 Si ratio in the ISM
has not significantly changed in the past 4.6 Gyr when the Sun
was born. In comparison, VY CMa and IRC+10216 were born
∼107 and 1−5 × 108 years ago, assuming masses of 25−32 and
3−5 M , respectively (see Portinari et al. 1998). We found stars
that we believe to be significantly older than the Sun, such as
W Hya (based on the mass-loss rate, initial mass, and current
age), to have lower 29 Si/30 Si ratios. For instance, with an initial
mass of 1−1.2 M , W Hya has an age of 5−10 Gyr. In either
the lower or higher age limit, this suggests a significant change
in the 29 Si/30 Si ratio between the pre- and post-solar period: the
29
Si/30 Si ratios in the ISM increase from about 1 to 1.5 between 5
to 10 Gyr ago and remain roughly constant after the Sun was
born. Given the time it takes low-mass stars to evolve onto the
AGBs, it is unlikely that many low-mass AGB stars existed in
our Galaxy between 5 and 10 Gyr ago, even if they had been
formed at the beginning of the Milky Way formation. It is therefore also unlikely that low-mass AGB stars were significant contributors to the GCE in the presolar era. The 29 Si/30 Si ratio in
the presolar era may be due to supernovae and/or other massive
29
Si/ 30 Si ratio in presolar grains
Assuming the 29 Si/30 Si ratio in the gas-phase SiO is the same
as it condenses onto dust grains or forms silicates, this primitive 29 Si/30 Si ratio may be carried by those grains when they
are incorporated into new stellar and planetary systems. The
29
Si/30 Si ratio in presolar SiC grains has been studied in some
meteorites (e.g., the Murchison meteorite, see the review by
Zinner 1998). They have been categorized into different types
(e.g., X, Y, and Z) according to their silicon isotopic anomalies. Most of the SiC grains found in meteorites are the so-called
mainstream grains (∼93%, see Fig. 3), i.e., those with a slope
of 1.34 on a silicon three-isotope plot (Hoppe et al. 1994). On
the other hand, SiO is expected to condense onto the dust formation regions near O-rich stars, or via a possible heteromolecular
nucleation of Mg, SiO, and H2 O to form silicates (Goumans &
Bromley 2012). In the studies of Si isotopes in primitive silicate
grains, the Si isotopic compositions of the majority of presolar silicates are similar to the SiC mainstream grains (Nguyen
et al. 2007; Mostefaoui & Hoppe 2004; Nagashima et al. 2004;
Vollmer et al. 2008), indicating that the amount of Si isotopes
locked in the SiC grains and the SiO group in silicates may
be similar; an example are the Orgueil silicate grains shown in
Fig. 3.
Most of the presolar grains have 29 Si/30 Si ratios around 1.5,
but evidence of lower 29 Si/30 Si ratios are also found in presolar
SiC grains, for instance, types X2 and Z in Fig. 3. The type Z
grains may have originated from a nearby evolved star (see also
Zinner et al. 2006). Additionally, the type X grains have been
proposed to have a supernova origin (e.g., Amari et al. 1992;
Hoppe et al. 1994), and have two or more subgroups (see, e.g.,
Hoppe et al. 1995; Lin et al. 2002) with possible different stellar origins. According to the study of Lin et al. (2002) on the
Qingzhen enstatite chondrite, the subgroups X1 and X2 show
somewhat similar N and O isotopes abundance ratios, but have
different slopes on the Si three-isotope plot (0.7 vs. 1.3 for X1
and X2, respectively). Because the metallicity in the local ISM is
increasing owing to the GCE, δ29 Si and δ30 Si will increase with
time accordingly. It is possible that the lower 29 Si/30 Si ratios seen
in X2 grains may have originated from a population of evolved
stars (such as the evolved stars with lower 29 Si/30 Si ratios). On
the other hand, X1 grains with higher 29 Si/30 Si ratios are likely to
be attributable to Type II supernovae (see also Zinner & Jadhav
2013). Moreover, it is important to point out that the higher-mass
(about 3 M ) evolved star sample from Tsuji et al. (1994) can be
well explained by the GCE (Fig. 3), considering the possible uncertainty in the 29 Si/30 Si ratio estimate for the present-day ISM.
L8, page 3 of 6
A&A 559, L8 (2013)
Fig. 3. Silicon three-isotope plot for presolar grains. The delta notation is defined as δi Si/28 Si = [(i Si/28 Si)/(i Si/28 Si) − 1] × 1000. The δ29 Si/δ30 Si
ratios do not translate directly into the 29 Si/30 Si ratios, which are plotted as black dashed lines. Left: the data of different subgroups (X, Y, and Z)
of SiC grains were taken from Lin et al. (2002), Amari et al. (2001), and Hoppe et al. (1997), and the Orgueil silicate grains from Zinner & Jadhav
(2013). The mainstream type (∼93%) of grains are indicated as a solid red line with a slope of 1.37. The dashed red line indicates the possible
extension from the mainstream grains to X2 grains. The filled triangle indicates the ISM value (Wolff 1980), and the black arrow indicates the
direction of the Galactic chemical evolution. The orange crosses are the evolved star sample (about 3 M ) from Tsuji et al. (1994). Right: similar
plot as the left one, but on a smaller scale, and the different silicate grain data were taken from Nguyen et al. (2007), Mostefaoui & Hoppe (2004),
and Nagashima et al. (2004).
4. Conclusions
We investigated the 29 Si/30 Si ratios of 15 evolved stars from
the thermal SiO isotopologue emission obtained by the APEX
and Herschel telescopes and from the literature. The inferred
29
Si/30 Si ratios tend to be lower among the older low-mass
O-rich stars. Because the 29 Si/30 Si ratios are not significantly
modified during the AGB phase and the contributions from the
low-mass AGB stars are less important due to their long lifetimes, the lower 29 Si/30 Si ratios imply different enrichment of
29
Si and 30 Si in the Galaxy between 5 to 10 Gyr ago with a nearly
constant value of 1.5 after that. Noting that presolar grains may
also have 29 Si/30 Si ratios lower than 1.5 (i.e., Type X2 and Z),
we suggest that these grains could have been produced by one
or more AGB stars with masses high enough to evolve onto the
AGB in time to contribute to presolar grains.
Acknowledgements. We thank the Swedish APEX staff for preparing observations and the referee for helpful comments. M.G.R. gratefully acknowledges support from the National Radio Astronomy Observatory (NRAO). The National
Radio Astronomy Observatory is a facility of the National Science Foundation
operated under cooperative agreement by Associated Universities, Inc. I.d.G.
acknowledges the Spanish MINECO grant AYA2011-30228-C03-01 (co-funded
with FEDER fund).
References
Alexander, C. M. O., & Nittler, L. R. 1999, ApJ, 519, 222
Amari, S., Hoppe, P., Zinner, E., & Lewis, R. S. 1992, ApJ, 394, L43
Amari, S., Nittler, L. R., Zinner, E., Lodders, K., & Lewis, R. S. 2001, ApJ, 559,
463
Anders, E., & Grevesse, N. 1989, Geochim. Cosmochim. Acta, 53, 197
Asplund, M., Grevesse, N., Sauval, A. J., & Scott, P. 2009, ARA&A, 47, 481
Cho, S.-H., & Ukita, N. 1998, AJ, 116, 2495
Choi, Y. K., Hirota, T., Honma, M., et al. 2008, PASJ, 60, 1007
De Beck, E., Decin, L., de Koter, A., et al. 2010, A&A, 523, A18
de Bièvre, P., Gallet, M., Holden, N. E., & Lynus Barnes, I. 1984, J. Phys. Chem.
Ref. Data, 13, 809
Decin, L., De Beck, E., Brünken, S., et al. 2010, A&A, 516, A69
Dorschner, J., & Henning, T. 1995, A&ARv, 6, 271
Gehrz, R. 1989, Interstellar Dust, 135, 445
Gilman, R. C. 1969, ApJ, 155, L185
Goumans, T. P. M., & Bromley, S. T. 2012, MNRAS, 420, 3344
Herwig, F. 2005, ARA&A, 43, 435
Hoppe, P., Amari, S., Zinner, E., Ireland, T., & Lewis, R. S. 1994, ApJ, 430, 870
Hoppe, P., Strebel, R., Pungitore, B., et al. 1995, Lunar and Planetary Institute
Science Conference Abstracts, 26, 621
Hoppe, P., Annen, P., Strebel, R., et al. 1997, ApJ, 487, L101
Iben, I., Jr., & Renzini, A. 1983, ARA&A, 21, 271
Justtanont, K., Khouri, T., Maercker, M., et al. 2012, A&A, 537, A144
Kim, H., Wyrowski, F., Menten, K. M., & Decin, L. 2010, A&A, 516, A68
Klein, B., Hochgürtel, S., Krämer, I., et al. 2012, A&A, 542, L3
Lebzelter, T., Posch, T., Hinkle, K., Wood, P. R., & Bouwman, J. 2006, ApJ, 653,
L145
Lin, Y., Amari, S., & Pravdivtseva, O. 2002, ApJ, 575, 257
Marigo, P., & Girardi, L. 2007, A&A, 469, 239
Mostefaoui, S., & Hoppe, P. 2004, ApJ, 613, L149
Nagashima, K., Krot, A. N., & Yurimoto, H. 2004, Nature, 428, 921
Nguyen, A. N., Stadermann, F. J., Zinner, E., et al. 2007, ApJ, 656, 1223
Penzias, A. A. 1981, ApJ, 249, 513
Portinari, L., Chiosi, C., & Bressan, A. 1998, A&A, 334, 505
Risacher, C., Vassilev, V., Monje, R., et al. 2006, A&A, 454, L17
Schöier, F. L., Ramstedt, S., Olofsson, H., et al. 2013, A&A, 550, A78
Timmes, F. X., & Clayton, D. D. 1996, ApJ, 472, 723
Tsuji, T., Ohnaka, K., Hinkle, K. H., & Ridgway, S. T. 1994, A&A, 289, 469
Ukita, N., & Kaifu, N. 1988, Atmospheric Diagnostics of Stellar Evolution, IAU
Colloq., 108, Lect. Notes Phys., 305, 51
Vassilev, V., Meledin, D., Lapkin, I., et al. 2008, A&A, 490, 1157
Vollmer, C., Hoppe, P., & Brenker, F. E. 2008, ApJ, 684, 611
Wolff, R. S. 1980, ApJ, 242, 1005
Woods, P. M., Schöier, F. L., Nyman, L.-Å., & Olofsson, H. 2003, A&A, 402,
617
Woosley, S. E., & Weaver, T. A. 1995, ApJS, 101, 181
Zhang, Y., Kwok, S., & Dinh-V-Trung 2009, ApJ, 691, 1660
Zhang, B., Reid, M. J., Menten, K. M., Zheng, X. W., & Brunthaler, A. 2012,
A&A, 544, A42
Zinner, E. 1998, Ann. Rev. Earth Planet. Sci., 26, 147
Zinner, E., & Jadhav, M. 2013, ApJ, 768, 100
Zinner, E., Nittler, L. R., Gallino, R., et al. 2006, ApJ, 650, 350
Zinner, E., Amari, S., Guinness, R., et al. 2007, Geochim. Cosmochim. Acta, 71,
4786
Pages 5 to 6 are available in the electronic edition of the journal at http://www.aanda.org
L8, page 4 of 6
T.-C. Peng et al.: Silicon isotopic abundance toward evolved stars
Fig. 4. Upper panels: APEX ground-vibrational 29 SiO (red) and 30 SiO (blue) J = 7−6 spectra toward o Ceti and R Leo. Lower panels:
Herschel/HIFI ground-vibrational 29 SiO (red) and 30 SiO (blue) J = 26−25 spectra at around 1.1 THz toward χ Cyg, R Cas, and R Dor. The
dashed lines indicate the VLSR of the sources.
Table 2. APEX and Herschel SiO integrated intensity measurements.
Source
VY CMa
R Cas
o Ceti
χ Cyg
R Dor
R Leo
W Hya
28
SiO 6–5
(K km s−1 )
107.4 ± 0.3
...
2.3 ± 0.1
...
...
...
18.4 ± 0.1
29
SiO 6–5
(K km s−1 )
24.8 ± 0.3
...
1.0 ± 0.1
...
...
...
4.8 ± 0.1
30
SiO 6–5
(K km s−1 )
16.3 ± 0.3
...
0.8 ± 0.1
...
...
...
4.3 ± 0.1
29
SiO 7–6
(K km s−1 )
...
...
1.2 ± 0.1
...
...
3.3 ± 0.1
...
30
SiO 7–6
(K km s−1 )
...
...
1.0 ± 0.1
...
...
2.5 ± 0.1
...
29
SiO 26–25
(K km s−1 )
10.1 ± 0.7
0.4 ± 0.1
0.9 ± 0.1
0.9 ± 0.1
3.2 ± 0.2
...
1.1 ± 0.1
30
SiO 26–25
(K km s−1 )
6.4 ± 0.3
0.3 ± 0.1
1.2 ± 0.1
0.8 ± 0.1
3.0 ± 0.2
...
1.2 ± 0.1
Notes. The integrated intensities are measured in T MB and do not include the calibration errors of the APEX and Herschel telescopes (from a few
per cent up to 10%) because the 29 SiO and 30 SiO lines were detected at the same band simultaneously and their ratios are not strongly affected by
the calibrations.
L8, page 5 of 6
A&A 559, L8 (2013)
Table 3. Overview of envelope terminal velocities, mass-loss rates, and 29 Si/30 Si ratios toward the selected evolved stars.
Source
d
(pc)
Ve
(km s−1 )
Ṁ
(M yr−1 )
VY CMa
NML Cyg
IRC+10216
IK Tau
TX Cam
CIT 6
G Her
R Cas
SW Vir
RX Boo
o Ceti
χ Cyg
R Dor
R Leo
W Hya
1170
1610
120
260
380
440
310
106
170
155
107
149
45
130
77
46.5
33.0
14.5
18.5
21.2
20.8
13.0
13.5
7.5
9.0
8.1
8.5
6.0
5.0
8.5
2.0 × 10−4
8.7 × 10−5
1.2 × 10−5
4.6 × 10−6
6.5 × 10−6
3.2 × 10−6
7.0 × 10−7
4.0 × 10−7
4.0 × 10−7
3.6 × 10−7
2.5 × 10−7
2.4 × 10−7
2.0 × 10−7
1.8 × 10−7
7.8 × 10−8
29
Si/30 Sia
1.55 ± 0.08
1.50 ± 0.20
1.46 ± 0.18
1.60 ± 0.30b
1.06 ± 0.54
0.95 ± 0.35
1.35 ± 0.31
1.09 ± 0.41
1.33 ± 0.32
1.31 ± 0.28
1.04 ± 0.06
1.06 ± 0.22c
1.14 ± 0.16
1.32 ± 0.04
0.99 ± 0.05
Spectral type
Stellar type
Note
M2/4II
M6I
C9,5e
M8/10IIe
M8.5
Ce
M6III
M7IIIe
M7III
M7.5e
M7e
S6
M8IIIe
M8IIIe
M7e
RSG
RSG
MIRA
MIRA
MIRA
SRa
SRb
MIRA
SRb
SRb
MIRA
MIRA
SRb
MIRA
SRa
APEX-1+HIFId
Tsuji et al. (1994)
Tsuji et al. (1994)
Decin et al. (2010); Kim et al. (2010)
Cho & Ukita (1998)
Zhang et al. (2009)
Tsuji et al. (1994)
HIFId
Tsuji et al. (1994)
Tsuji et al. (1994)
APEX-1/2+HIFId
HIFId
HIFId
APEX-2d
APEX-1+HIFI d
Notes. The data of distance d, terminal velocity of CO envelope Ve , and mean mass-loss rate Ṁ of the selected sources were compiled from Woods
et al. (2003), De Beck et al. (2010), Justtanont et al. (2012), and Schöier et al. (2013). We note that Schöier et al. (2013) adopted smaller distances
for χ Cyg (110 pc) and RX Boo (120 pc), and the distance to VY CMa was averaged from two measurements (Choi et al. 2008; Zhang et al. 2012).
The mean 29 Si/30 Si ratios for VY CMa, o Ceti, and W Hya were derived from the thermal 29 SiO/30 SiO emission ratios obtained by the APEX and
Herschel telescopes. The 29 Si/30 Si ratios for R Cas, χ Cyg, and R Dor were derived from the Herschel/HIFI data. The 29 Si/30 Si ratios of G Her,
SW Vir, and RX Boo were taken from Tsuji et al. (1994), TX Cam from Cho & Ukita (1998), and CIT 6 from Zhang et al. (2009). Spectral types
were taken from the SIMBAD database, De Beck et al. (2010), and the references therein. (a) The 29 Si/30 Si ratios are the mean values (equally
weighted) when more than one transition was detected. (b) The Herschel/HIFI data only show a 2-σ detection of 29 SiO and 30 SiO J = 26−25 lines
with a ratio of 1.6 ± 0.8. However, judging from the APEX J = 8−7 and 7−6 data of Kim et al. (2010), the integrated ratios are also close to 1.6.
We note that the baselines in the 30 SiO spectra of Kim et al. (2010) may be too low. Therefore, the actual 29 SiO/30 SiO ratio should be 1.6 (see
also the discussion of Decin et al. 2010, who adopted an abundance ratio of 3 ± 2 from their modeling results). (c) The ratio reported by Ukita &
Kaifu (1988) and Tsuji et al. (1994) is about 2.4 with a large uncertainty (same as V1111 Oph) estimated from J = 2−1, which may be affected
by masing effects. Therefore, we estimated the 29 SiO/30 SiO ratio only from the new HIFI measurements. (d) The SiO intensity measurements are
listed in Table 2.
L8, page 6 of 6